Recurrent CME-like eruptions in emerging flux regions. II. Scaling of energy and collision of successive eruptions

P. Syntelis, V. Archontis, K. Tsinganos

Research output: Contribution to journalArticlepeer-review

3 Citations (Scopus)

Abstract

We present results of three-dimensional MHD simulations of recurrent eruptions in emerging flux regions. The initial numerical setup is the same as that in the work by Syntelis et al. Here, we perform a parametric study on the magnetic field strength (B 0) of the emerging field. The kinetic energy of the produced ejective eruptions in the emerging flux region ranges from 1026 to 1028 erg, reaching up to the energies of small coronal mass ejections. The kinetic and magnetic energies of the eruptions scale linearly in a logarithmic plot. We find that the eruptions are triggered earlier for higher B 0 and that B 0 is not directly correlated to the frequency of occurrence of the eruptions. Using large numerical domains, we show the initial stage of the partial merging of two colliding erupting fields. The partial merging occurs partly by the reconnection between the field lines of the following and the leading eruption at the interface between them. We also find that tether-cutting reconnection of the field lines of the leading eruption underneath the following eruption magnetically links the two eruptions. Shocks develop inside the leading eruption during the collision.
Original languageEnglish
Article number61
Number of pages8
JournalAstrophysical Journal
Volume876
Issue number1
DOIs
Publication statusPublished - 3 May 2019

Keywords

  • Magnetohydrodynamics (MHD)
  • Methods: numerical
  • Sun: activity
  • Sun: interior
  • Sun: magnetic fields

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